Solar flares are sudden and violent releases of magnetic energy in the solar atmosphere and can be divided as eruptive flares, when plasma is ejected from the solar atmosphere, resulting in a CME , and as confined flares when no CME is associated with the flare ([1]}; [2]}).
In addition to full and failed eruptions, there are cases where only a part of the filament is erupted, such events are defined as partial erupting events. Partial eruption may or may not be associated with a CME ([3]}; [4]}; [5]}; [6]}; [7]}). The most energetic flares are commonly eruptive ([8]}), even though confined, non-eruptive X-class flares have been reported ([9]}; [10]}; [11]}) as well as CMEs with associated only C-class flares ([12]}; [13]}).
